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Big and young SMBHs in the early Universe: how ...

Big and young SMBHs in the early Universe: how can we observe jetted AGN?

Talk at "Quasars at all cosmic epochs", held in Padova (2-7 April 2017)

Tullia Sbarrato

April 07, 2017
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  1. Big and Young SMBHs 
 in the early Universe Tullia

    Sbarrato Università Milano - Bicocca
  2. Big and Young SMBHs 
 in the early Universe Tullia

    Sbarrato Università Milano - Bicocca how can we observe jetted AGN?
  3. ✓b = 1/ ✓v ✓v < 1/ 2 2 ⇠

    340 450 viewing angle: analogous jetted AGN, randomly oriented: Why blazars? Padova, 7 April 2017
  4. ✓b = 1/ ✓v ✓v < 1/ 2 2 ⇠

    340 450 viewing angle: analogous jetted AGN, randomly oriented: Why blazars? Padova, 7 April 2017
  5. ✓b = 1/ ✓v ✓v < 1/ 2 2 ⇠

    340 450 viewing angle: analogous jetted AGN, randomly oriented: Why blazars? Padova, 7 April 2017 Tagliaferri et al. 2015
  6. High-z jetted quasars Padova, 7 April 2017 blazars can be

    found in optical quasar catalogs: SDSS+FIRST quasar catalog 105783 z > 4 1248 radio-detected (>1mJy) 53 radio loudness > 100 31
  7. Blazar classification Padova, 7 April 2017 Gamma-ray observations do not

    help X-ray observations! Sbarrato et al. 2012; 2013b
  8. blazars can be found in optical quasar catalogs: SDSS+FIRST quasar

    catalog 105783 z > 4 1248 radio-detected (>1mJy) 53 radio loudness > 100 31 blazars (up to now!) 8 High-z jetted quasars M > 109M Padova, 7 April 2017
  9. blazars can be found in optical quasar catalogs: SDSS+FIRST quasar

    catalog 105783 z > 4 1248 radio-detected (>1mJy) 53 radio loudness > 100 31 blazars (up to now!) 8 High-z jetted quasars M > 109M 2700 jetted quasars 2 2 Padova, 7 April 2017
  10. blazars can be found in optical quasar catalogs: SDSS+FIRST quasar

    catalog 105783 z > 4 1248 radio-detected (>1mJy) 53 radio loudness > 100 31 blazars (up to now!) 8 High-z jetted quasars M > 109M 2700 jetted quasars 2  Fblazar Flim 1/p 1 2 2 Padova, 7 April 2017 140 slightly misaligned
  11. Ghisellini et al. 2014 UCMB / (1 + z)4 CMB

    energy density at z~3 becomes competitive with magnetic energy density in quasar lobes radio emission is quenched! CMB quenching Padova, 7 April 2017
  12. Ghisellini & TS, 2016 Ld = ⌘d ˙ Mc2 ⌘

    = ⌘d + ⌘B Which form first? Padova, 7 April 2017
  13. Summary • two different formation epochs for early jetted and

    non-jetted AGN: jetted sources form first! • we do not see the “parents” of aligned jetted AGN:
 - CMB quenching of extended radio emission?
 - heavy nuclear obscuration (dark bubbles)? we are likely missing many high-z jetted sources! Padova, 7 April 2017